三维MHD天体层模型观测量的天图
Skymaps of observables of three-dimensional MHD astrosphere models
摘要：
天体球的三维模型最近引起了人们的兴趣。然而，由于观测的二维性质，这些模型和观测之间的比较是不平凡的。通过将选定的天体球三维模型的物理值投影到以虚拟全天观测者为中心的球体表面上，这些模型可以与不同观测量的观测数据进行比较：柱密度、韧致辐射通量、旋转测量、H $α$通量和同步加速器或回旋加速器通量。投影的计算方法是将天体球模型旋转和移动到所需的位置和方向，然后用修正的视线积分法计算球体上某块区域的值。考虑了由所讨论的视线连接到贴片的所有模型单元对所选择的可观察量的贡献。当模型产生弓形激波时，在投影的每一个观测点上都可以看到由外鞘产生的明显的抛物线结构，确切的形状取决于视线和恒星运动的方向。在所有四个被检查的天体层模型中，只有$λ$ Cephei的模型显示的通量高于目前的观测阈值。这是由于$λ$造父变星模型中强烈的恒星风和星际流入。
英文摘要：
Three-dimensional models of astrospheres have recently become of interest. However, comparisons between these models and observations are non-trivial because of the two-dimensional nature of observations. By projecting selected physical values of three-dimensional models of astrospheres onto the surface of a sphere that is centred on a virtual all-sky observer, these models can be compared to observational data in different observables: the column density, bremsstrahlung flux, rotation measure, H$α$ flux, and synchrotron or cyclotron flux. Projections were calculated by rotating and moving the astrosphere model to the desired position and orientation and by then computing the value of a given patch on the sphere by a modified line-of-sight integration. Contributions to the selected observable made by all model cells that are connected to the patch by the line of sight in question were taken into account. When the model produces a bow shock, a distinct parabolic structure produced by the outer astrosheath can be seen in every observable of the projection, the exact shape depending on the orientations of the line of sight and the stellar motion. Of all four examined astrosphere models, only that of $λ$ Cephei shows fluxes that are higher than current observational thresholds. This is due to the strong stellar wind and interstellar inflow of the $λ$ Cephei model.
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